The WAC global mosaic is comprised of over 15,000 images acquired
between November 2009 and February 2011. The WAC maps the whole Moon
in one month, however the solar incidence angle at the equator changes
about 28° from the beginning to the end of the month. To even out
the incidence angle variations, the mosaic is comprised of data
collected over three periods (1/20/2010 to 1/28/2010, 5/30/2010
to 6/6/2010, 7/24/2010 to 7/31/2010) (Table 1). Some gores were filled
with data taken at other times. The non-polar images were map projected
onto the GLD100 (WAC derived 100m/pixel DTM)
while polar images were map projected on the LOLA shape model
(80° to 90° N/S) and the GLD100 (60° to 80° N/S).
Accurate positioning of each WAC image was ensured using ephemeris
provided by the LOLA and GRAIL team and an improved camera geometry model
(Speyerer,
E.J. et al, 2014, Pre-flight and On-orbit Geometric Calibration of the Lunar
Reconnaissance Orbiter Camera). To reduce brightness discrepancies
across image boundaries, all images were corrected to a common photometric
geometry using a Hapke model
(Sato, H.
et al, 2014, Resolved Hapke parameter maps of the Moon). This mosaic uses
only the 643 nm band of the WAC.

The WAC global mosaic is archived in ten regional tiles at three
different resolutions: 100 meters/pixel, 256 pixels/degree, and
128 pixels/degree. Eight of the tiles are equirectangular projections
that encompass 60° latitude by 90° longitude (for the 128
pixels/degree products, these tiles extend from the equator to the pole).
In addition, polar stereographic projections are available for each
pole from 60° to the pole.